CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


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George Mason University (USA) - University of Michigan (USA) - University of Cambridge (UK)


CHIANTI consists of a critically evaluated set of up-to-date atomic data, together with user-friendly programs written in Interactive Data Language (IDL) and Python to calculate the spectra from astrophysical plasmas.

The CHIANTI package is freely available.
If you use the package, we only ask you to appropriately acknowledge CHIANTI .




- The Chianti wine-producing area of Tuscany, Italy -

CHIANTI Database Version 7.1.4 released on May 20, 2014

The splups file for Fe XXI, which included the electron impact effective collision strengths, was inadvertently missing some data for collisional excitation from levels 4 and 5 of the ground configuration to higher levels. This omission caused level populations for these two levels to be inaccurate at densities above about 10^13 cm^-3.

The A-values for the O II 1-5 transition 2s2.2p3 4S1.5-2s2.2p3 2P1.5 at 2471.09A and the 1-4 2s2.2p3 4S1.5-2s2.2p3 2P0.5 at 2470.97A were found to be reversed.

The file containing the parameters for dielectronic recombination for Al II, al_2.drparams, had become corrupted. The file has been repaired and a new ionization balance file has been calculated. The error mainly affected the ionization balance of Al I and Al II.

CHIANTI Version 7.1 released

The main feature of CHIANTI Version 7.1 is the inclusion of a large number of configurations to the atomic models of Fe VIII to XIV. These configurations give rise to a forest of spectral lines in the 50-170 A wavelength range that contribute significantly to the total radiative output of the Sun at those wavelengths. Also, they give rise to several strong lines that are currently neglected by spectral codes, and provide significant contributions to the SDO/AIA bandpasses centered at 94A and 131A. These data are calculated using the Flexible Atomic Code (FAC) under the distorted wave approximation. Additional data for a few more ions are included, that improve the available datasets for a few ions, and correct a few glitches for other ions at all wavelength ranges. New element abundance data sets are provided, and improved recombination rates are included and used to provide a new set of CHIANTI ionization equilibria (chianti.ioneq file).

We are grateful to individual scientists and funding agencies for their support.